Entry and Acceleration of Solar Wind Electrons in the Earth's Outer Magnetosphere

Details Entry and Acceleration of Solar Wind Electrons in the Earth's Outer Magnetosphere Entry and Acceleration of Solar Wind Electrons in the Earth's Outer Magnetosphere

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh42a0484s&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH42A-0484

Physics

Plasma Physics

2100 Interplanetary Physics, 2400 Ionosphere, 2700 Magnetospheric Physics, 7500 Solar Physics, Astrophysics, And Astronomy, 7800 Space Plasma Physics

Scientific paper

It is well known that during the recovery of magnetic storms, relativistic electron fluxes are usually enhanced over pre-storm values in the inner magnetosphere near geosynchronous orbit. Although the final acceleration of electrons to MeV energies most likely occurs in the inner magnetosphere, observations indicate that an enhanced flux of energized electrons (> 10 keV) forms in the so-called seed region located at about 10 RE radially from the Earth in the equatorial plane. To examine the acceleration of electrons from the solar wind to the seed region, a study is being undertaken whereby electron trajectories are followed starting upstream of the bow shock, through the magnetopause and throughout the outer magnetosphere. The entry locations of electrons will be examined along with acceleration mechanisms that occur between the solar wind and seed region. The electron particle trajectories are followed based on the guiding center approximation in a global MHD model of the solar wind interaction with the Earth's magnetosphere for various interplanetary magnetic field (IMF) conditions.

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